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A fundamental parameter in star formation is the primordial multiplicity fraction. It has been argued, on the one hand, that most stars form in binary or higher order systems; and on the other that the majority of stars form as singles. It is widely accepted that most, if not all stars form in clusters. I present simulations of the dynamical evolution of a typical (Orion-like) cluster to examine the effects on the primordial multiplicity and the separation distribution of those stars that do form in multiple systems. I compare these results with the current observed properties of stars in the field and attempt to infer the initial parameters of a typical star forming region.
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