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The star forming
ability of an unbound GMC was investigated recently,
reporting that not only is star formation efficiency
(SFE) low in such a cloud, but the ensemble of clusters within the cloud can
resemble an OB associations. Here, we present a more detailed set of
calculations which are intended to build upon this earlier work. The new
simulations compare both the cloud's dynamical state and the equation of state
on its ability to form clusters. Our motivation with these calculations is to
establish whether the internal conditions of a GMC can significantly alter the
manner in which the star formation occurs, such as the SFE, the star formation
rate, and the cluster separations and dynamics. In keeping with spirit of this
meeting, we also present a list of flaws with our simulation, and one final
simulation in which the GMC is "forming" from a large scale shock in an attempt
at more realistic initial conditions. This final simulation gives at least some
measure of the limitations of our method.
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