  We have undertaken a series of hydrodynamic + N-body simulations in order to
explore the properties of young stars. Our results suggest that the IMF may be
sensitive to environment in its substellar region, with more brown dwarfs being
formed where clusters are denser or more compact. We find that multiple stars
are a natural outcome of collapsing turbulent flows, with a high incidence of N
> 2 multiples. We find a positive correlation of multiplicity with primary mass
but a companion frequency that decreases with age. Binary brown dwarfs are
rarely formed, in conflict with observations. Brown dwarfs as companions are
predominantly found orbiting binaries or triples at large separations.
