The stellar content of H72.97-69.39, a potential super star cluster in
  the making
  Young Massive Clusters (YMCs) and Super Star Clusters (SSCs) represent an
extreme mode of star formation. Far-infrared imaging of the Magellanic Clouds
has identified one potential embedded SSC, HSO BMHERICC J72.971176-69.391112
(HH in short), in the south-west outskirts of the Large Magellanic Cloud. We
present Gemini Flamingos 2 and GSAOI near-infrared imaging of a 3'x3' region
around HH in order to characterize the stellar content of the cluster. The
stellar content is probed down to 1.5 Msun. We find substantial dust extinction
across the cluster region, extending up to A_K of 3. Deeply embedded stars are
associated with ALMA-detected molecular gas suggesting that star formation is
ongoing. The high spatial resolution of the GSAOI data allows identification of
the central massive object associated with the 13CO ALMA observations and to
detect fainter low-mass stars around the H30alpha ALMA source. The morphology
of the molecular gas and the nebulosity from adjacent star formation suggest
they have interacted covering a region of several pc. The total stellar content
in the cluster is estimated from the intermediate- and high-mass stellar
content to be at least 10000 Msun, less than R136 with up to 100 000 Msun
within 4.7 pc radius, but places it in the regime of a super star cluster.
Based on the extinction determination of individual stars we estimate a
molecular gas mass in the vicinity of HH of 6600 Msun, suggesting more star
formation can be expected.
