The chapter reviews the current understanding of star formation, emphasizing the role of turbulence in creating and counteracting gravitational forces. It discusses the key dynamical processes—turbulence, magnetic fields, and self-gravity—and their nonlinear and multidimensional interactions. The authors use physical arguments and numerical simulations to explain the features and scalings involved in star formation, dividing the process into large-scale and small-scale regimes. Large-scale processes include the formation and evolution of giant molecular clouds (GMCs) and their substructures, while small-scale processes involve dense cores and protostellar systems. The chapter covers the formation of low- and high-mass stars, the development of winds and outflows, and the mechanisms governing angular momentum transport in disks. Despite remaining questions, the framework is now in place to build a comprehensive theory of star formation, which will be tested by future telescopes.The chapter reviews the current understanding of star formation, emphasizing the role of turbulence in creating and counteracting gravitational forces. It discusses the key dynamical processes—turbulence, magnetic fields, and self-gravity—and their nonlinear and multidimensional interactions. The authors use physical arguments and numerical simulations to explain the features and scalings involved in star formation, dividing the process into large-scale and small-scale regimes. Large-scale processes include the formation and evolution of giant molecular clouds (GMCs) and their substructures, while small-scale processes involve dense cores and protostellar systems. The chapter covers the formation of low- and high-mass stars, the development of winds and outflows, and the mechanisms governing angular momentum transport in disks. Despite remaining questions, the framework is now in place to build a comprehensive theory of star formation, which will be tested by future telescopes.