tokens: which suffers from persistence and non-linearity effects, we created pixel-to-pixel maps that we used to pre-process and correct the raw images (details in Section A ). Following standard data reduction steps (Section 2.1 ) and calibration, we were able to achieve excellent image registration resulting in a sharp and stable PSF of 0.25 arcsec over the entire 4 × 4 arcmin LUCI 2 field of view. The PSF size only increases by out to the detector edges (Section B ). This superb spatial resolution enables to resolve the star cluster candidates and bring down contamination from background galaxies to a minimum. In a forthcoming paper we will present the detailed analysis of the star cluster system of NGC 6384 (cf Section 3.1 ), while in this paper we mainly focus our analysis to the central 3.6 × 3.6 kpc (∼36 × 36 arcsec) overlap region between our NIR LBT and archival optical HST data. The high spatial NIR imaging is crucial for breaking age–metallicity–reddening degeneracies when combined with the optical HST data. We reprocessed the HST /ACS and WFPC 2 data to the same plate scale resolution of 0.05 arcsec pixel −1 (cf. Section 2.2 ). We performed a 2D MCMC image fitting with imfit (Erwin 2015 ) by using a PSF model built from stars in the image for both the LUCI 2 and HST images, as well as a tinytim (Krist et al. 2011 ) PSF model drizzled in identical manner as the science images. We also used a pixel mask of the central obscuring disc-like dust lane (Section 3.2 , Fig. 5 ). Our main findings can be summarizes as follows: We uncover the presence of two inner Sersić (low n − index, disc?) components (Section 3.2 , Fig. 4 and Section 4.1 ) with effective radii of ∼100 and 400 pc in which the NSC with r eff ≃ 10 pc is embedded. NGC 6384 has a large-scale boxy bulge (∼1 kpc) and disc (∼6 kpc). The effective radius of NGC 6384 NSC increases with wavelength (cf. Fig. 11 , which suggests for a more centrally concentrated younger stellar population (see Section 4.2 ). The NSC effective radius is smaller in size by and magnitude/mass by ∼0.4 mag/dex compared to Georgiev Böker ( 2014 ) due to the unaccounted inner Sersić components. This highlights the need to resolve and model well the central regions for the correct mass and dynamical modelling of the NSC when follow-up spectroscopy is included. The NSC SED is described by an old population (10.8 ± 1.3 Gyr) with a stellar mass of , and a young population of 230 ± 140 Myr, which is of its mass. Both populations have slightly sub- and supersolar metallicity, respectively (cf. Table 2 , Sections 3.3 and 4.3 ). We obtained the SED radial surface mass density, age, metalicity, and reddening (cf. Fig 10 , Sections 3.3 and 4.3 ) We find negligible, 1 per cent fraction of the light, to be coming from a weak AGN (Section 4.4 ). If an MBH in the NSC of NGC 6384 is present, then it might not be accreting, similarly to those in the MW and M 31. All structural and stellar population evidences suggest that the NGC
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