  Cygnus X is one of the closest and most active high-mass star-forming regions
in our Galaxy, making it one of the best laboratories for studying massive star
formation. As part of the GLOSTAR Galactic plane survey, we performed large
scale simultaneous H$_{2}$CO (1$_{1,0}$-1$_{1,1}$) spectral line and radio
continuum imaging observations toward Cygnus X at $\lambda\sim$6 cm with the
Karl G. Jansky Very Large Array and the Effelsberg-100 m radio telescope. Our
Effelsberg observations reveal widespread H$_{2}$CO (1$_{1,0}$-1$_{1,1}$)
absorption with a spatial extent of $\gtrsim$50 pc in Cygnus~X for the first
time. On large scales of 4.4 pc, the relative orientation between local
velocity gradient and magnetic field tends to be more parallel at H$_{2}$
column densities of $\gtrsim$1.8$\times 10^{22}$~cm$^{-2}$. On the smaller
scale of 0.17 pc, our VLA+Effelsberg combined data reveal H$_{2}$CO absorption
only toward three bright H{\scriptsize II} regions. Our observations
demonstrate that H$_{2}$CO (1$_{1,0}$-1$_{1,1}$) is commonly optically thin.
Kinematic analysis supports the assertion that molecular clouds generally
exhibit supersonic motions on scales of 0.17-4.4 pc. We show a non-negligible
contribution of the cosmic microwave background radiation in producing extended
absorption features in Cygnus X. Our observations suggest that H$_{2}$CO
($1_{1,0}-1_{1,1}$) can trace molecular gas with H$_{2}$ column densities of
$\gtrsim 5 \times 10^{21}$ cm$^{-2}$. The ortho-H$_{2}$CO fractional abundance
with respect to H$_{2}$ has a mean value of 7.0$\times 10^{-10}$. A comparison
of velocity dispersions on different linear scales suggests that the dominant
$-3$ km s$^{-1}$ velocity component in the prominent DR21 region has nearly
identical velocity dispersions on scales of 0.17-4.4 pc, which deviates from
the expected behavior of classic turbulence.
