  The initial sizes and masses of massive star clusters provide information
about the cluster formation process and also determine how cluster populations
are modified and destroyed, which have implications for using clusters as
tracers of galaxy assembly. Young massive cluster populations are often assumed
to be unchanged since cluster formation, and therefore their distribution of
masses and radii are used as the initial values. However, the first few hundred
million years of cluster evolution does change both cluster mass and cluster
radius, through both internal and external processes. In this paper, we use a
large suite of $N$-body cluster simulations in an appropriate tidal field to
determine the best initial mass and initial size distributions of young
clusters in the nearby galaxy M83. We find that the initial masses follow a
power-law distribution with a slope of -2.7 $\pm$ 0.4, and the half-mass radii
follow a log-normal distribution with a mean of 2.57 $\pm$ 0.04 pc and a
dispersion of 1.59 $\pm$ 0.01 pc. The corresponding initial projected
half-light radius function has a mean of 2.7 $\pm$ 0.3 pc and a dispersion of
1.7 $\pm$ 0.2 pc. The evolution of the initial mass and size distribution
functions are consistent with mass loss and expansion due to stellar evolution,
independent of the external tidal field and the cluster's initial density
profile. Observed cluster sizes and masses should not be used as the initial
values, even when clusters are only a few hundred million years old.
