  We have studied the system of globular clusters (GCs) that formed in other
galaxies and eventually accreted onto the Milky Way. Thus, the samples of GCs
belonging to different tidal streams, obtained on the basis of the latest data
from the Gaia observatory, were taken from the literature. We measured the
anisotropy of the distribution of these GCs using the gyration tensor and found
that the distribution of GCs in the streams is isotropic. Nevertheless, it can
be seen that some of the accreted GCs included into existing samples actually
belong to the disk of the Galaxy. To clarify the origin of GCs, we investigated
the ``age--metallicity'' relation. This dependence demonstrates bimodality and
its two different branches clearly show the difference between the clusters
formed in the streams and in the disk of the Galaxy. Furthermore, we have
studied the influence of the large--scale environment of the Galaxy (i.e., the
Local Supercluster) on the distribution of satellite galaxies and Galactic GCs.
The satellite galaxies of the Milky Way are known to form an anisotropic planar
structure, so we included them in our analysis too. An inspection has shown
that the plane of the satellite galaxies is perpendicular both to the disk of
the Galaxy and the supergalactic plane. For GCs more distant than 100~Kpc, a
similar picture is observed.
