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Despite their importance as stellar nurseries and the building blocks ofgalaxies, very little is known about the formation of the highest massclusters. The dense clump G0.253+0.016 represents an example of a clump thatmay form an Arches-like, high-mass cluster. Here we present molecular line mapstoward G0.253+0.016 taken as part of the MALT90 molecular line survey,complemented with APEX observations. Combined, these data reveal the globalphysical properties and kinematics of G0.253+0.016. Recent Herschel data showthat while the dust temperature is low (~19 K) toward its centre, the dusttemperature on the exterior is higher (~27 K) due to external heating. Our newmolecular line data reveal that, overall, the morphology of dense gas detectedtoward G0.253+0.016 matches very well its IR extinction and dust continuumemission. An anti-correlation between the dust and gas column densities towardits centre indicates that the clump is centrally condensed with a cold, denseinterior in which the molecular gas is chemically depleted. The velocity fieldshows a strong gradient along the clump's major axis, with the blue-shiftedside at higher Galactic longitude. The optically thick gas tracers aresystematically red-shifted with respect to the optically thin and hot gastracers, indicating radial motions. The gas kinematics and line ratios supportthe recently proposed scenario in which G0.253+0.016 results from a tidalcompression during a recent pericentre passage near SgrA*. Because G0.253+0.016represents an excellent example of a clump that may form a high-mass cluster,its detailed study should reveal a wealth of knowledge about the early stagesof cluster formation.

G0.253+0.016: A centrally condensed, high-mass protocluster