tokens: took advantage of recent studies that thoroughly examined the LMC cluster population in some selected fields located within the B17 's surveyed area. Fig. 2 shows the distribution of the B17 's objects and the seven well-studied LMC regions considered here overplotted. The large hexagons correspond to DECam fields (∼2° × 2° FOV, pixel size = 0.263 arcsec; Flaugher et al. 2015 ) analysed by Piatti ( 2017c ), while the small rectangles correspond to MOSAIC II fields (36 arcmin×36 arcmin FOV, pixel size = 0.269 arcsec) studied by Piatti ( 2017b ) and Piatti et al. ( 2018 ). The 4-m Blanco telescope at the Cerro Tololo Interamerican Observatory (CTIO) was employed to observe those fields, among others distributed outwards the B17 's surveyed area as part of different photometric surveys aimed at studying the most metal-poor stars outside the Milky Way (rectangles: CTIO 2008B-0296 programme; PI: Cole) and the Magellanic Clouds stellar history (hexagons; Nidever et al. 2017 ). Figure 2. Spatial distribution of B17 's objects with selected LMC fields studied by Piatti ( 2017c ) (hexagons) and Piatti ( 2017b ) and Piatti et al. ( 2018 ) (rectangles) overplotted. These LMC fields were carefully surveyed looking for star clusters by employing the method mentioned above (Piatti et al. 2016 ), i.e. by constraining the search using the known cluster dimension and mean stellar density ranges. The final cluster lists resulted to be statistically complete, because the derived photometry detected any star cluster based on counts of its brightest stars all the way down to the main-sequence turnoff (MSTO) of the oldest LMC clusters. Every catalogued B08 's cluster was recovered, in addition to very few new identified clusters in some of the surveyed fields. The CMDs of the recognized extended objects were then cleaned from field star contamination by using the procedure developed by Piatti Bica ( 2012 ), i.e. by building statistically meaningful star field CMDs that tightly reproduced the luminosity function, colour distribution, and stellar density of the respective star fields, to be subtracted to the cluster CMDs. The resulting cleaned CMDs for some of the objects led to conclude that they are not genuine physical systems, but random fluctuations of the field star density. Table 1 lists the number of entries in the B08 's catalogue for each selected LMC field (field ID is as in Fig. 2 ), and the number of true star clusters confirmed according to the photometric analyses performed by Piatti ( 2017c , 2017b ) and Piatti et al. ( 2018 ). Table 1. Statistics of star clusters in LMC fields. Ref.: 1) Piatti ( 2017c ); 2) Piatti ( 2017b ); 3) Piatti et al. ( 2018 ). For comparison purposes, we extracted the results of Section 2 for the selected LMC fields, namely, the number of B08 's objects matched by the B17 's ones as well as the number of B17 's new detections. They are also listed in Table 1 . For completeness, we included in its last column the deprojected
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