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In this paper we present the distribution of molecular gas in the Milky WayGalactic plane from $l$ = [59.75, 74.75]$^{\circ}$ and $b$ = [${-}$5.25,+5.25]$^{\circ}$, using the MWISP $^{12}$CO/$^{13}$CO/$\rm {C}^{18}{O}$emission line data. The molecular gas in this region can be mainly attributedto the Local spur, Local arm, Perseus arm, and Outer arm. Statistics of thephysical properties of the molecular gas in each arm, such as excitationtemperature, optical depth, and column density, are presented. Using the DBSCANalgorithm, we identified 15 extremely distant molecular clouds with kinematicdistances of 14.72$-$17.77 kpc and masses of 363$-$520 M$_{\odot}$, which wefind could be part of the Outer Scutum-Centaurus (OSC) arm identified by\cite{2011ApJ...734L..24D} and \cite{2015ApJ...798L..27S}. It is also possiblethat, 12 of these 15 extremely distant molecular clouds constitute anindependent structure between the Outer and the OSC arms or a spur. There existtwo Gaussian components in the vertical distribution of the molecular gas inthe Perseus spiral arm. These two Gaussian components correspond to two giantfilaments parallel to the Galactic plane. We find an upward warping of themolecular gas in the Outer spiral arm with a displacement of around 270 pc withrespect to the Galactic mid-plane.

Molecular Clouds in the Galactic Plane from $l$ = [59.75$^\circ$, 74.75$^\circ$] and $b$ = [$-$5.25$^\circ$, +5.25$^\circ$]