  The [CII] 158 $\mu$m emission line and the underlying far-infrared (FIR) dust
continuum are important tracers for studying star formation and kinematic
properties of early galaxies. We present a survey of the [CII] emission lines
and FIR continua of 31 luminous quasars at $z>6.5$ using the Atacama Large
Millimeter Array (ALMA) and the NOrthern Extended Millimeter Array (NOEMA) at
sub-arcsec resolution. This survey more than doubles the number of quasars with
[CII] and FIR observations at these redshifts and enables statistical studies
of quasar host galaxies deep into the epoch of reionization. We detect [CII]
emission in 27 quasar hosts with a luminosity range of $L_{\rm
[CII]}=(0.3-5.5)\times10^9~L_\odot$ and detect the FIR continuum of 28 quasar
hosts with a luminosity range of $L_{\rm FIR}=(0.5-13.0)\times10^{12}~L_\odot$.
Both $L_{\rm [CII]}$ and $L_{\rm FIR}$ are correlated ($\rho\simeq0.4$) with
the quasar bolometric luminosity, albeit with substantial scatter. The quasar
hosts detected by ALMA are clearly resolved with a median diameter of $\sim$5
kpc. About 40% of the quasar host galaxies show a velocity gradient in [CII]
emission, while the rest show either dispersion-dominated or disturbed
kinematics. Basic estimates of the dynamical masses of the rotation-dominated
host galaxies yield $M_{\rm dyn}=(0.1-7.5)\times10^{11}~M_\odot$. Considering
our findings alongside those of literature studies, we found that the ratio
between $M_{\rm BH}$ and $M_{\rm dyn}$ is about ten times higher than that of
local $M_{\rm BH}-M_{\rm dyn}$ relation on average but with substantial scatter
(the ratio difference ranging from $\sim$0.6 to 60) and large uncertainties.
