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We present a detailed 3D kinematic analysis of the central regions ($R<30''$)of the low-mass and dynamically evolved galactic globular cluster NGC 6362. Thestudy is based on data obtained with ESO-VLT/MUSE used in combination with theadaptive optics module and providing $\sim3000$ line-of-sight radialvelocities, which have been complemented with Hubble Space Telescope propermotions. The quality of the data and the number of available radial velocitiesallowed us to detect for the first time a significant rotation signal along theline of sight in the cluster core with amplitude of $\sim 1$ km/s and with apeak located at only $\sim20''$ from the cluster center, corresponding to only$\sim10\%$ of the cluster half-light radius. This result is further supportedby the detection of a central and significant tangential anisotropy in thecluster innermost regions. This is one of the most central rotation signalsever observed in a globular cluster to date. We also explore the rotationalproperties of the multiple populations hosted by this cluster and find thatNa-rich stars rotate about two times more rapidly than the Na-poorsub-population thus suggesting that the interpretation of the present-dayglobular cluster properties require a multi-component chemo-dynamical approach.Both the rotation amplitude and peak position would fit qualitatively thetheoretical expectations for a system that lost a significant fraction of itsoriginal mass because of the long-term dynamical evolution and interaction withthe Galaxy. However, to match the observations more quantitatively furthertheoretical studies to explore the initial dynamical properties of the clusterare needed.

3D core kinematics of NGC$~$6362: central rotation in a dynamically evolved globular cluster