  We present observations of CO(3-2) and $^{13}$CO(3-2) emission near the
supernebula in the dwarf galaxy NGC 5253, which contains one of the best
examples of a potential globular cluster in formation. The 0.3" resolution
images reveal an unusual molecular cloud, "Cloud D1", coincident with the
radio-infrared supernebula. The ~6-pc diameter cloud has a linewidth, $\Delta$
v = 21.7 km/s, that reflects only the gravitational potential of the star
cluster residing within it. The corresponding virial mass is 2.5 x 10$^5$
M$_\odot$. The cluster appears to have a top-heavy initial mass function, with
$M_{low}$~1-2 M$_\odot$. Cloud D1 is optically thin in CO(3-2) probably because
the gas is hot. Molecular gas mass is very uncertain but constitutes < 35% of
the dynamical mass within the cloud boundaries. In spite of the presence of an
estimated ~1500-2000 O stars within the small cloud, the CO appears relatively
undisturbed. We propose that Cloud D1 consists of molecular clumps or cores,
possibly star-forming, orbiting with more evolved stars in the core of the
giant cluster.
