Abstract
Star formation involves a complex interplay of supersonic turbulence, magnetic fields, stellar feedback, and gravity. While observations yield empirical rules, it is difficult to formulate a comprehensive theory of star formation. Open questions include the inefficiency of star formation, as well as the origins of stellar clustering. Numerical simulations present a bridge between theory and observations. In this talk, I will present previous results from a suite of magnetohydrodynamics (MHD) simulations of star formation from giant molecular clouds (GMCs), aimed at quantifying the influence of turbulent and magnetic support on star formation efficiency and molecular cloud destruction. I will then discuss my current research on protostellar disk fragmentation as a possible mechanism for the formation of bound multiple stellar systems.