  We present simulations of the dynamical evolution of young embedded star
clusters. Our initial conditions are directly derived from X-ray, infrared, and
radio observations of local systems, and our models evolve both gas and stars
simultaneously. Our regions begin with both clustered and extended
distributions of stars, and a gas distribution which can include a filamentary
structure in addition to gas surrounding the stellar subclusters. We find that
the regions become spherical, monolithic, and smooth quite quickly, and that
the dynamical evolution is dominated by the gravitational interactions between
the stars. In the absence of stellar feedback, the gas moves gently out of the
centre of our regions but does not have a significant impact on the motions of
the stars at the earliest stages of cluster formation. Our models at later
times are consistent with observations of similar regions in the local
neighbourhood. We conclude that the evolution of young proto-star clusters is
relatively insensitive to reasonable choices of initial conditions. Models with
more realism, such as an initial population of binary and multiple stars and
ongoing star formation, are the next step needed to confirm these findings.
