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The initial sizes and masses of massive star clusters provide informationabout the cluster formation process and also determine how cluster populationsare modified and destroyed, which have implications for using clusters astracers of galaxy assembly. Young massive cluster populations are often assumedto be unchanged since cluster formation, and therefore their distribution ofmasses and radii are used as the initial values. However, the first few hundredmillion years of cluster evolution does change both cluster mass and clusterradius, through both internal and external processes. In this paper, we use alarge suite of $N$-body cluster simulations in an appropriate tidal field todetermine the best initial mass and initial size distributions of youngclusters in the nearby galaxy M83. We find that the initial masses follow apower-law distribution with a slope of -2.7 $\pm$ 0.4, and the half-mass radiifollow a log-normal distribution with a mean of 2.57 $\pm$ 0.04 pc and adispersion of 1.59 $\pm$ 0.01 pc. The corresponding initial projectedhalf-light radius function has a mean of 2.7 $\pm$ 0.3 pc and a dispersion of1.7 $\pm$ 0.2 pc. The evolution of the initial mass and size distributionfunctions are consistent with mass loss and expansion due to stellar evolution,independent of the external tidal field and the cluster's initial densityprofile. Observed cluster sizes and masses should not be used as the initialvalues, even when clusters are only a few hundred million years old.

The Initial Properties of Young Star Clusters in M83