  Stripped-envelope (SE) supernovae (SNe) include H-poor (Type IIb), H-free
(Type Ib) and He-free (Type Ic) events thought to be associated with the deaths
of massive stars. The exact nature of their progenitors is a matter of debate.
Here we present the analysis of the light curves of 34 SE SNe published by the
Carnegie Supernova Project (CSP-I), which are unparalleled in terms of
photometric accuracy and wavelength range. Light-curve parameters are estimated
through the fits of an analytical function and trends are searched for among
the resulting fit parameters. We found a tentative correlation between the peak
absolute $B$-band magnitude and $\Delta m_{15}(B)$, as well as a correlation
between the late-time linear slope and $\Delta m_{15}$. Making use of the full
set of optical and near-IR photometry, combined with robust host-galaxy
extinction corrections, bolometric light curves are constructed and compared to
both analytic and hydrodynamical models. From the hydrodynamical models we
obtained ejecta masses of $1.1-6.2$ $M_{\odot}$, $^{56}$Ni masses of
$0.03-0.35$ $M_{\odot}$, and explosion energies (excluding two SNe Ic-BL) of
$0.25-3.0\times10^{51}$ erg. Our analysis indicates that adopting $\kappa =
0.07$ cm$^{2}$ g$^{-1}$ as the mean opacity serves to be a suitable assumption
when comparing Arnett-model results to those obtained from hydrodynamical
calculations. We also find that adopting He I and O I line velocities to infer
the expansion velocity in He-rich and He-poor SNe, respectively, provides
ejecta masses relatively similar to those obtained by using the Fe II line
velocities. The inferred ejecta masses are compatible with intermediate mass
($M_{ZAMS} \leq 20$ $M_{\odot}$) progenitor stars in binary systems for the
majority of SE SNe. Furthermore, the majority of our SNe is affected by
significant mixing of $^{56}$Ni, particularly in the case of SNe Ic.
