  N-body simulations are used to model the early evolution of globular
clusters. These simulations include residual gas which was not turned into
stars which is expelled from the globular cluster by the actions of massive
stars. The results of these simulations are compared to observations of 8 LMC
globular clusters less than 100 Myr old. These observations are used to
constrain the initial conditions that may have produced these clusters. It is
found that the entire variety of young LMC globular clusters may be explained
in a model where they form from a fairly uniform population of roughly
spherical, relaxed proto-cluster clouds very similar to Giant Molecular Clouds
in the Galaxy, with star formation efficiencies between 25% and 60%. This paper
has been accepted for publication in MNRAS.
