  We compare properties of classical and pseudo-bulges and properties of their
hosting galaxies selected from the MaNGA survey. Bulge types are identified
based on the S$\mathrm{\acute{e}}$rsic index n of bulge component and the
position of bulges on the Kormandy diagram. For the 393 classical bulges and
422 pseudo-bulges selected and their hosting galaxies, we study their kinematic
properties including a proxy for specific angular momentum and central velocity
dispersion, their stellar population properties including stellar age,
metallicity, and specific star formation rate, as well as HI fractions of the
galaxies. Our results show that at given stellar mass, disc components of
pseudo-bulge galaxies are younger, have more active star formation, rotate
more, and may contain more HI content compared with those of classical bulge
galaxies, and the differences are larger than those between bulges themselves.
The correlations between bulge types and disc properties indicate that
different types of bulges are shaped by different processes that may regulate
both growth of central components and evolution of outer discs in galaxies. In
addition, we propose a stellar mass dependent divider of central velocity
dispersion to separate galaxies with classical bulges from those with
pseudo-bulges in galaxy mass range of $10.4<\mathrm{log}(M_*/M_\odot)<11.4$:
$\mathrm{log}(\sigma_0) = 0.23 \times \mathrm{log}(M_*/M_\odot)-0.46$. Galaxies
with larger/smaller $\sigma_0$ can be classified as hosts of
classical/pseudo-bulges.
