  The number of known globular clusters in the Galactic bulge has been
increasing steadily thanks to different new surveys. The aim of this study is
to provide a census of the newly revealed globular clusters in the Galactic
bulge, and analyze their characteristics. In recent years, many globular
clusters have been discovered or identified. The stellar populations to which
they belong are indicated in their original studies: they are mostly bulge
clusters, with some identified as disk or halo members. We collected 41 new
globular clusters revealed in the last decade and compared them to the known
bulge clusters. The new clusters are intrinsically faint with $M_V$ of around
-6.0 mag. The distance to the Sun of the ensemble of well-known and new bulge
clusters is compatible with the Galactocentric distance measurements from the
Galactic black hole location. The ensemble sample shows metallicity peaks at
[Fe/H] ~ -1.08 $\pm$ 0.35 and -0.51 $\pm$ 0.25 dex, confirming previous
findings. The age-metallicity relation of the new clusters younger than 10 Gyr
is compatible with that of the ex situ samples of the dwarf galaxies
Sagittarius, Canis Majoris, and Gaia-Enceladus-Sausage. The clusters with ages
between 11.5 and 13.5 Gyr show no age-metallicity relation, because they are
all old. This is compatible with their formation in situ in the early Galaxy.
