  We reconstruct the initial two-body relaxation time at the half mass radius
for a sample of young $\aplt 300$ Myr star clusters in the large Magellanic
cloud. We achieve this by simulating star clusters with 12288 to 131072 stars
using direct $N$-body integration. The equations of motion of all stars are
calculated with high precision direct $N$-body simulations which include the
effects of the evolution of single stars and binaries. We find that the initial
relaxation times of the sample of observed clusters in the large Magellanic
cloud ranges from about 200 Myr to about 2 Gyr. The reconstructed initial
half-mass relaxation times for these clusters has a much narrower distribution
than the currently observed distribution, which ranges over more than two
orders of magnitude.
