  We present the results of a series of numerical simulations of compressible,
self-gravitating hydrodynamic turbulence of cluster-forming clumps in molecular
clouds. We examine the role that turbulence has in the formation of
gravitationally bound cores, studying the dynamical state, internal structure
and bulk properties of these cores. Complex structure in turbulent clumps is
formed provided that the damping time of the turbulence, $t_{damp}$ is longer
than the gravitational free-fall time $t_{ff}$ in a region. We find a variety
of density and infall velocity structures among the cores in the simulation,
including cores that resemble the Larson-Penston collapse of an isothermal
sphere ($\rho \propto r^{-2}$) as well as cores that resemble the
McLaughlin-Pudritz collapse of logatropic spheres ($\rho \propto r^{-1}$). The
specific angular momentum profiles range between $j \propto r^{1} - r^{2}$. The
masses of the bound cores that form are well-fit by the turbulent mass spectrum
of Padoan and Nordlund (2002), while the specific angular momentum distribution
can be fit by a broken power law. While our hydrodynamic simulations reproduce
many of the observed properties of cores, we find an upper limit for the star
formation efficiency (SFE) in clusters of 40-50 per cent.
