Simulations predict that intermediate-mass black holes (IMBHs) can form in globular clusters (GCs) during star formation. IMBHs have masses between 100 and 10⁵ solar masses (M☉). Previous simulations suggested that mergers of black holes within GCs could only produce IMBHs below 500 M☉ due to gravitational wave recoil. However, new simulations show that high-density star formation in the parent giant molecular cloud of a GC can lead to sufficient mergers of massive stars, allowing IMBHs with masses above 10³ M☉ to form. These IMBHs are massive enough to remain in the GC despite gravitational wave recoil. IMBHs are less well understood than stellar-mass and supermassive black holes. Observations suggest that some IMBHs may exist in GCs, with masses between 10³ and 10⁴ M☉. Theoretical models suggest that IMBHs could form through the merger of binary black holes or via the collapse of very massive stars (VMSs) in dense stellar environments. However, VMSs in GCs may lose mass through stellar winds, limiting their ability to form massive IMBHs. Simulations of GC formation show that VMSs can form through runaway collisions in dense star clusters. These VMSs can then merge to form IMBHs. The mass of these IMBHs depends on the star formation rate and the metallicity of the cluster. Simulations indicate that IMBHs with masses above 10³ M☉ can form in GCs with masses up to 10⁶ M☉. The mass of the IMBH is also influenced by the metallicity of the cluster, with higher metallicity leading to lower IMBH masses due to increased mass loss from stellar winds. Theoretical models suggest that the mass accumulation rate of VMSs is about 3% of the star formation rate of the cluster. This rate is influenced by the collision rate and the average mass of colliding stars. The mass of the IMBH is determined by the balance between mass accumulation and mass loss from stellar winds. Simulations show that IMBHs with masses above 10³ M☉ can form in GCs with masses up to 10⁶ M☉, and these IMBHs are likely to remain in the GC despite gravitational wave recoil. Observational estimates of IMBH masses in GCs align with simulation results. The mass of IMBHs in GCs is influenced by the initial mass and metallicity of the cluster. Simulations suggest that IMBHs with masses up to 10⁴ M☉ can form in GCs with masses up to 10⁶ M☉. However, higher metallicity GCs may not host as massive IMBHs due to increased mass loss from stellar winds. The simulations also show that the rotation of GCs isSimulations predict that intermediate-mass black holes (IMBHs) can form in globular clusters (GCs) during star formation. IMBHs have masses between 100 and 10⁵ solar masses (M☉). Previous simulations suggested that mergers of black holes within GCs could only produce IMBHs below 500 M☉ due to gravitational wave recoil. However, new simulations show that high-density star formation in the parent giant molecular cloud of a GC can lead to sufficient mergers of massive stars, allowing IMBHs with masses above 10³ M☉ to form. These IMBHs are massive enough to remain in the GC despite gravitational wave recoil. IMBHs are less well understood than stellar-mass and supermassive black holes. Observations suggest that some IMBHs may exist in GCs, with masses between 10³ and 10⁴ M☉. Theoretical models suggest that IMBHs could form through the merger of binary black holes or via the collapse of very massive stars (VMSs) in dense stellar environments. However, VMSs in GCs may lose mass through stellar winds, limiting their ability to form massive IMBHs. Simulations of GC formation show that VMSs can form through runaway collisions in dense star clusters. These VMSs can then merge to form IMBHs. The mass of these IMBHs depends on the star formation rate and the metallicity of the cluster. Simulations indicate that IMBHs with masses above 10³ M☉ can form in GCs with masses up to 10⁶ M☉. The mass of the IMBH is also influenced by the metallicity of the cluster, with higher metallicity leading to lower IMBH masses due to increased mass loss from stellar winds. Theoretical models suggest that the mass accumulation rate of VMSs is about 3% of the star formation rate of the cluster. This rate is influenced by the collision rate and the average mass of colliding stars. The mass of the IMBH is determined by the balance between mass accumulation and mass loss from stellar winds. Simulations show that IMBHs with masses above 10³ M☉ can form in GCs with masses up to 10⁶ M☉, and these IMBHs are likely to remain in the GC despite gravitational wave recoil. Observational estimates of IMBH masses in GCs align with simulation results. The mass of IMBHs in GCs is influenced by the initial mass and metallicity of the cluster. Simulations suggest that IMBHs with masses up to 10⁴ M☉ can form in GCs with masses up to 10⁶ M☉. However, higher metallicity GCs may not host as massive IMBHs due to increased mass loss from stellar winds. The simulations also show that the rotation of GCs is