  A mass function of small-scale dark matter clumps is calculated in the
standard cosmological scenario with an inflationary-produced primordial
fluctuation spectrum and with a hierarchical clustering. We take into account
the tidal destruction of clumps at early stages of structure formation starting
from a time of clump detachment from the Universe expansion. Only a small
fraction of these clumps, ~0.1-0.5%, in each logarithmic mass interval
$\Delta\log M\sim1$ survives the stage of hierarchical clustering. The
surviving clumps can be disrupted further in the galaxies by tidal interactions
with stars. We performed the detailed calculations of the tidal destruction of
clumps by stars in the Galactic bulge and halo and by the Galactic disk itself.
It is shown that the Galactic disc provides the dominant contribution to the
tidal destruction of small-scale clumps outside the bulge. The results obtained
are crucial for calculations of the dark matter annihilation signal in the
Galaxy.
