  The kinematics of about 2000 classical Cepheids of the Milky Way with data
from Gaia\,EDR3 catalog has been studied. For some of these stars, there are
line-of-sight velocities. On the basis of the nonlinear rotation model, the
parameters of the rotation curve of the Galaxy were determined. The circular
linear rotation velocity of the near-solar neighborhood around the Galaxy
center was $V_0=236\pm 3$~km s$^{-1}$ for the assumed Sun's galactocentric
distance $R_0=8.1\pm0.1$~kpc. Analysis of residual velocities of Cepheids based
on the linear Ogorodnikov-Milne model showed the presence of the following
significantly different from zero gradients: $\partial U/\partial x,$ $\partial
U/\partial z,$ $\partial V/\partial x,$ $\partial V/\partial z$ and $\partial
W/\partial x,$ which behaves differently depending on the selection radius. The
most interesting is the gradient $\partial W/\partial x\sim-0.5\pm0.1$~km
s$^{-1}$ kpc$^{-1}$ (positive rotation of this star system around the galactic
axis $y$, $\Omega_y$) since the velocities $W$ are free of galactic rotation.
Here we have an indirect influence of various effects leading to a perturbation
of the vertical velocities of the galactic disk stars. Based on a simpler
model, a more accurate estimate of this rotation is obtained,
$\Omega_y=0.51\pm0.07$~km s$^{-1}$ kpc$^{-1}$.
