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NGC 4382 is a merger-remnant galaxy that has been classified as morphological type E2, S0, and even Sa. In this work, we performed a photometric and spectroscopic analysis of the globular cluster (GC) system of this peculiar galaxy in order to provide additional information about its history. We used a combination of photometric data in different filters, and multi-object and long-slit spectroscopic data obtained using the Gemini/GMOS instrument. The photometric analysis of the GC system, using the Gaussian Mixture Model algorithm in the colour plane, reveals a complex colour distribution within $R_\mathrm{gal}<5$ arcmin (26.1 kpc), showing four different groups: the typical blue and red subpopulations, a group with intermediate colours, and the fourth group towards even redder colours. From the spectroscopic analysis of 47 GCs, confirmed members of NGC\,4382 based on radial velocities, we verified 3 of the 4 photometric groups from the analysis of their stellar populations using the ULySS code. NGC 4382 presents the classic blue ($10.4\pm2.8$ Gyr, $\mathrm{[Fe/H]}=-1.48\pm0.18$ dex) and red ($12.1\pm2.3$ Gyr, $\mathrm{[Fe/H]}=-0.64\pm0.26$ dex) GCs formed earlier in the lifetime of the galaxy, and a third group of young GCs ($2.2\pm0.9$ Gyr; $\mathrm{[Fe/H]}=-0.05\pm0.28$ dex). Finally, analysis of long-slit data of the galaxy reveals a luminosity-weighted mean age for the stellar population of $\sim$2.7 Gyr, and an increasing metallicity from [Fe/H]=$-0.1$ to $+0.2$ dex in $R_\mathrm{gal}<10$ arcsec (0.87 kpc). These values, and other morphological signatures in the galaxy, are in good agreement with the younger group of GCs, indicating a common origin as a result of a recent merger.