The study investigates the formation of intermediate-mass black holes (IMBHs) in globular clusters (GCs). Previous simulations have shown that IMBHs with masses up to 500 solar masses (M⊙) cannot be formed due to gravitational wave recoil during mergers. However, the authors perform detailed star-by-star simulations of GC formation, considering high-density star formation in the parent giant molecular clouds (GMCs). They find that the high stellar density in GMCs can lead to sufficient mergers of massive stars, overcoming the mass threshold for IMBH formation. The simulations predict that GCs can form IMBHs with masses of at least 1000 M⊙, which are large enough to be retained within the GC even with the expected gravitational wave recoil. The results suggest that IMBHs with masses up to 1000 M⊙ can be formed in GCs, providing a possible explanation for the observed properties of IMBHs in these systems. The study also compares the predicted IMBH masses with observational estimates and discusses the fate of IMBHs in GCs, suggesting that low-metallicity GCs may still host IMBHs.The study investigates the formation of intermediate-mass black holes (IMBHs) in globular clusters (GCs). Previous simulations have shown that IMBHs with masses up to 500 solar masses (M⊙) cannot be formed due to gravitational wave recoil during mergers. However, the authors perform detailed star-by-star simulations of GC formation, considering high-density star formation in the parent giant molecular clouds (GMCs). They find that the high stellar density in GMCs can lead to sufficient mergers of massive stars, overcoming the mass threshold for IMBH formation. The simulations predict that GCs can form IMBHs with masses of at least 1000 M⊙, which are large enough to be retained within the GC even with the expected gravitational wave recoil. The results suggest that IMBHs with masses up to 1000 M⊙ can be formed in GCs, providing a possible explanation for the observed properties of IMBHs in these systems. The study also compares the predicted IMBH masses with observational estimates and discusses the fate of IMBHs in GCs, suggesting that low-metallicity GCs may still host IMBHs.