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[abridged] We report a series of simulations of the formation of a starcluster similar to the Orion Nebula Cluster (ONC), including both radiativetransfer and protostellar outflows, and starting from both smooth andself-consistently turbulent initial conditions. Each simulation forms >150stars and brown dwarfs, yielding a stellar mass distribution from < 0.1 to > 10Msun. We show that a simulation that begins with self-consistently turbulenceembedded in a larger turbulent volume, and that includes protostellar outflows,produces an initial mass function (IMF) consistent both with that of the ONCand the Galactic field. This is the first simulation published to date thatreproduces the observed IMF in a cluster large enough to contain massive stars,and where the result is determined by a fully self-consistent calculation ofgas thermodynamics. This simulation also produces a star formation rate that,while still somewhat too high, is much closer to observed values than if weomit either the larger turbulent volume or the outflows. Moreover, we show thatthe combination of outflows, self-consistently turbulent initial conditions,and turbulence continually fed by motions on scales larger than that of theprotocluster yields an IMF that is in agreement with observations and invariantwith time, resolving the "overheating" problem in which simulations withoutthese features have an IMF peak that shifts to progressively higher masses overtime. The simulation that matches the observed IMF also reproduces the observedtrend of stellar multiplicity strongly increasing with mass. We show that thissimulation produces massive stars from distinct massive cores whose propertiesare consistent with those of observed massive cores. However, the stars formedin these cores also undergo dynamical interactions that naturally produceTrapezium-like hierarchical multiple systems.

Radiation-Hydrodynamic Simulations of the Formation of Orion-Like Star Clusters II. The Initial Mass Function from Winds, Turbulence, and Radiation