  The differences in the relationships between the physical parameters and the
chemical-element abundances in accreted globular star clusters and those formed
inside the Galaxy have been investigated. The information on the supposed
formation sites of the clusters based on the Gaia~DR2 data is borrowed from the
literature. Those sources estimate the probability of belonging to the Galactic
bulge and disk, as well as to six known events of the merger of dwarf satellite
galaxies with the Milky Way, for 151~globular clusters. It is shown that all
metal-poor ($\rm{[Fe/H]}<-1.0$) genetically related globular clusters have high
relative abundances of $\alpha$-elements. According to modern views, since type
II supernovae release more $\alpha$-elements into the interstellar medium with
increasing mass, it has been suggested that masses of type II supernovae in the
Galaxy were greater than in the accreted galaxies. It is proved that the
clusters of the low-energy group, which were considered accreted, are
genetically related to a single protogalactic cloud, same as the unstratified
clusters UKS~1 and Liller~1, which most likely belong to the bulge. It is shown
that not only the lower but also the upper limits of the clusters' masses
decrease with an increase in the average radius of their orbits. The latter
fact is explained by a decrease in the masses of emerging clusters with a
decrease in the masses of their host galaxies. It is demonstrated that an
extremely multicomponent stellar population is observed only in accreted
globular clusters with an initial mass $>10^{6}M_{\odot}$. It has been
suggested that these clusters retained all the matter ejected by their evolved
stars, from which new generations of stars formed due to long evolution far
from our Galaxy.
