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Globular clusters (GCs) are the most ancient stellar systems in the MilkyWay. Therefore, they play a key role in the understanding of the early chemicaland dynamical evolution of our Galaxy. Around $40\%$ of them are placed within$\sim4$ kpc from the Galactic center. In that region, all Galactic componentsoverlap, making their disentanglement a challenging task. With Gaia DR2, wehave accurate absolute proper motions for the entire sample of known GCs thathave been associated with the bulge/bar region. Combining them with distances,from RR Lyrae when available, as well as radial velocities from spectroscopy,we can perform an orbital analysis of the sample, employing a steady Galacticpotential with a bar. We applied a clustering algorithm to the orbitalparameters apogalactic distance and the maximum vertical excursion from theplane, in order to identify the clusters that have high probability to belongto the bulge/bar, thick disk, inner halo, or outer halo component. We foundthat $\sim 30\%$ of the clusters classified as bulge GCs based on theirlocation are just passing by the inner Galaxy, they appear to belong to theinner halo or thick disk component, instead. Most of GCs that are confirmed tobe bulge GCs are not following the bar structure and are older than the epochof the bar formation.

Globular clusters in the inner Galaxy classified from dynamical orbital criteria