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We present the stellar radial velocity analysis of the central 1x1' of theyoung massive Small Magellanic Cloud star cluster NGC 346. Using VLT/MUSEintegral field spectroscopy in combination with Hubble Space Telescopephotometry we extract 103 spectra of cluster member stars suited to measureaccurate line-of-sight kinematics. The cluster member stars show two distinctvelocity groups at v1 = -3.3 (+0.3/-0.2) km/s and v2 = 2.6 (+0.1/-0.1) km/s,relative to the systemic velocity of 165.5+/-0.2 km/s, and hint for a thirdgroup at v3 = 9.4 (+0.1/-0.1 km/s. We show that there is neither a correlationbetween the velocity groups and the spatial location of the stars, nor theirlocus on optical color-magnitude diagrams, which makes the stellar velocity akey parameter to separate individual stellar components in such a young starcluster. Velocity group 2 shows clear rotation with Omega2 = -0.4 +/- 0.11/Myr, corresponding to -4.9+/-0.7 km/s at radial distance of 10 pc from thecenter, a possible remnant of the formation process of NGC 346 through thehierarchical collapse of the giant molecular cloud. The ionizing gas has lostany natal kinematic imprint and shows clear expansion, driven by far ultraviolet fluxes and stellar winds of the numerous OB stars in the cluster center.The size of this expanding bubble and its expansion velocity of 7.9 km/s is inexcellent agreement with the estimate that the latest star formation episodeoccurred about two million years ago.

The internal line-of-sight kinematics of NGC 346: the rotation of the core region