  The surface brightness profiles of globular clusters are conventionally
described with the well-known King profile. However, observations of young
massive clusters (YMCs) in the local Universe suggest that they are better fit
by simple models with flat central cores and simple power-law densities in
their outer regions (such as the Elson-Fall-Freeman, or EFF, profile).
Depending on their initial central density, these YMCs may also facilitate
large numbers of stellar collisions, potentially creating very massive stars
that will directly collapse to intermediate-mass black holes (IMBHs). Using
Monte Carlo $N$-body models of YMCs, we show that EFF-profile clusters
transform to Wilson or King profiles through natural dynamical evolution, but
that their final $W_0$ parameters do not strongly correlate to their initial
concentrations. The most centrally-dense YMCs can produce runaway stellar
mergers as massive as $4000\,M_{\odot}$ (the largest resolved mass in our
simulations) which can collapse to produce IMBHs of similar masses. In doing
so, these runaway collisions also deplete the clusters of their primordial
massive stars, reducing the number of stellar-mass BHs by as much as $\sim$
40\%. This depletion will accelerate the core collapse of clusters, suggesting
that the process of IMBH formation itself may produce the high densities
observed in some core-collapsed clusters.
