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Star clusters are the birthplace of most stars, yet our understanding
of their formation and early evolution during the gas-dominated phase
remains poor. This is especially so for massive, >
10^4 M_sun clusters, of which there are few nearby examples.
We present deep VLT/HAWKI imaging of a gas-dominated,
massive, young star-forming clump. With a total gas mass
of 2x10^4 M_sun and an infall rate of
~3.4x10^{-2} M_sun/yr$, the clump is potentially a
progenitor of massive star clusters like NGC 3603. Due to its relative
proximity of 2.5kpc we can probe the full stellar initial mass
function in the early stages of star formation. We map the
projected two dimensional structure of the cluster and compare it to
the gas distribution in order to distinguish between fast and slow
formation, based on the amount of sub-structure observed.
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