  I present measurements of the projected rotational velocities of a sample of
100 early B-type main-sequence stars in the Large Magellanic Cloud. This is the
first extragalactic study of the distribution of stellar rotational velocities.
The sample is drawn from two sources: a sample derived from the vicinity of the
main-sequence turnoff of young clusters (ages 1-3x10^7yrs), and a sample from
the general field. I find the cluster population exhibits significantly more
rapid rotation than that seen in the field. I have drawn analogous Galactic
cluster and field samples from the literature. Comparison of these samples
reveals the same effect. I propose the observed difference between cluster and
field populations can be explained by a scenario of evolutionary enhancement of
the surface angular momentum over the main-sequence lifetime. A comparison is
made between the cluster and field populations of the LMC and the Galaxy in
order to explore the effects of metallicity. This shows that the LMC stars are
more rapid rotators than their Galactic counterparts.
