  Many globular clusters (GCs) in the Milky Way (MW) have been studied in
recent years, especially in hidden regions such as those of the Galactic bulge.
Our main goal is to understand what we can learn if we include these new
objects into the MWGC system that we know today. We catalogue 37 recently
discovered GCs. We use different distributions for investigating the MWGC
system: metallicity distribution (MD), luminosity function (LF), and age
distribution. We first treat separately the new GCs sample from the known and
well-characterised GCs. We merge these two samples, upgrading the MWGC system.
We performed a comparison between our clusters sample and field star (FS)
population. We find a double peaked distribution for the LF, which shows an
elongated faint end tail. Considering the "merged" sample, the LF and the MDs
display a bimodality trend. We construct the MD for the FS sample, and
comparing this with that one of the GCs, we learn that a high percentage of FS
show [Fe/H]$>0$, whereas we do not detect any GCs in the same metallicity
range. In order to understand this inconsistency, we construct the
age-metallicity diagram for both samples, noting that the old and metal-poor
population (age$\geq8$ Gyr and [Fe/H]$\leq -1.0$) is represented by GCs, while
the young and metal-rich population (age$<8$ Gyr and [Fe/H]$>-1.0$) corresponds
to FS. From the analysis of the GC LF and MD, we can conclude that many GCs,
probably those very faint, have survived strong dynamical processes, typical of
the Bulge regions. We cannot exclude the possibility that some of them have
been accreted during past merging events, especially the metal-poor component,
whereas the metal-rich population may be related to the formation of the bulge
and/or disk. Finally, the difference that we notice between the GC and FS
samples should be sought in the evolutionary difference between these two
stellar populations.
