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Analyzing the dynamical state of nearby young massive star clusters isessential understanding star cluster formation and evolution during theirearliest stages. In this work we analyze the stellar and gas kinematics of theyoung massive star cluster Westerlund 2 (Wd2) using data from the integralfield unit MUSE and complement them with proper motions from the Gaia DR2. Themean gas radial velocity of $15.9\,{\rm km}\,{\rm s}^{-1}$ agrees with theassumption that Wd2 is the result of a cloud-cloud collision. The gas motionsshow the expansion of the HII region, driven by the radiation from the many OBstars in the cluster center. The velocity profile of the cluster member starsreveal an increasing velocity dispersion with decreasing stellar mass and thatthe low-mass stars show five distinct velocity groups. Based on their spatialcorrelation with the cluster's two clumps, we concluded that this is theimprint of the initial cloud collapse that formed Wd2. A thorough analysis ofthe dynamical state of Wd2, which determines a dynamical mass range of $M_{\rmdyn,Wd2} = (7.5 \pm 1.9)\cdot10^4 - (4.4 \pm 1.1)\cdot10^5\,{\rm M}_\odot$ andexceeds the photometric mass by at least a factor of two leads to theconclusion that Wd2 is not massive enough to remain gravitationally bound.Additionally we also identify 22 runaway candidates with peculiar velocitiesbetween 30 and $546\,{\rm km}\,{\rm s}^{-1}$.

The young massive star cluster Westerlund 2 observed with MUSE. III. A cluster in motion -- the complex internal dynamics