  We have studied the properties of molecular clouds in the second quadrant of
the Milky Way Mid-plane from l$=$104$.\!\!^{\circ}$75 to
l$=$119$.\!\!^{\circ}$75 and b$=-$5$.\!\!^{\circ}$25 to b$=$5$.\!\!^{\circ}$25
using the $^{12}$CO, $^{13}$CO, and C$^{18}$O $J=1-0$ emission line data from
the Milky Way Imaging Scroll Painting project (MWISP). We have identified 857
and 300 clouds in the $^{12}$CO and $^{13}$CO spectral cubes, respectively,
using the DENDROGRAM + SCIMES algorithms. The distances of the molecular clouds
are estimated and the physical properties like masses, sizes, and surface
densities of the clouds are tabulated. The molecular clouds in the Perseus arm
are about 30$-$50 times more massive and 4$-$6 times larger than the clouds in
the Local arm. This result, however, is likely biased by distance selection
effects. The surface densities of the clouds are enhanced in the Perseus arm
with an average value of $\sim$100 M$_{\odot}$ pc$^{-2}$. We selected the 40
most extended ($>$0.35 arcdeg$^2$) molecular clouds from the $^{12}$CO catalog
to build the H$_2$ column density probability distribution function (N-PDF).
About 78\% of the N-PDFs of the selected molecular clouds are well fitted with
log-normal functions with only small deviations at high-densities which
correspond to star-forming regions with scales of $\sim$1-5 pc in the Local arm
and $\sim$5-10 pc in the Perseus arm. About 18\% of the selected molecular
clouds have power-law N-PDFs at high-densities. In these molecular clouds, the
majority of the regions fitted with the power-law correspond to molecular
clumps of sizes of $\sim$1 pc or filaments of widths of $\sim$1 pc.
