  We study the physical properties and 3D distribution of molecular clouds
(MCs) toward the Cygnus region using the MWISP CO survey and Gaia DR3 data.
Based on Gaussian decomposition and clustering for $\rm ^{13}CO$ lines, over
70% of the fluxes are recovered. With the identification result of $\rm
^{13}CO$ structures, two models are designed to measure the distances of the
molecular gas in velocity crowding regions. The distances of more than 200
large $\rm ^{13}CO$ structures are obtained toward the 150 square degree
region. Additionally, tens of the identified MC structures coincide well with
masers and/or intense mid-IR emission. We find multiple gas layers toward the
region: (1) the extensive gas structures composing the Cygnus Rift from 700 pc
to 1 kpc across the whole region; (2) the $\sim$ 1.3 kpc gas layer mainly in
the Cygnus X South region; and (3) the 1.5 kpc dense filament at the Cygnus X
North region and many cometary clouds shaped by Cygnus OB2. We also note that
the spatial distribution of YSO candidates is generally consistent with the
molecular gas structures. The total molecular mass of the Cygnus region is
estimated to be $\sim 2.7\times10^{6}~M_{\odot}$ assuming an X-factor ratio
$X_{\rm CO} = 2 \times 10^{20} \rm cm^{-2} (K\cdot km\cdot s^{-1})^{-1}$. The
foreground Cygnus Rift contributes $\sim$25% of the molecular mass in the whole
region. Our work presents a new 3D view of the MCs' distribution toward the
Cygnus X region, as well as the exact molecular gas mass distribution in the
foreground Cygnus Rift.
