  One of the problem revealed recently in cosmology is a so-called Hubble
tension (HT), which is the difference between values of the present Hubble
constant, measured by observation of the universe at redshift $z \lesssim 1$,
and by observations of a distant universe with CMB fluctuations originated at
$z \sim 1100$. In this paper we suggest, that this discrepancy may be explained
by deviation of the cosmological expansion from a standard Lambda-CDM %simple
Friedman model of a flat universe, during the period after recombination at $z
\lesssim 1100$, due to action of additional variable component of a dark energy
of different origin.. We suppose, that a dark matter (DM) has a common origin
with a variable component of a dark energy (DEV). DE presently may have two
components, one of which is the Einstein constant $\Lambda$, and another,
smaller component DEV ($\Lambda_V$) comes from the remnants of a scalar fields
responsible for inflation. Due to common origin and interconnections the
densities of DEV and DM are supposed to be connected, and remain almost
constant during, at least, the time after recombination, when we may
approximate $\rho_{DM}=\alpha \rho_{DEV}$. This part of the dark energy in not
connected with the cosmological constant $\Lambda$, but is defined by existence
of scalar fields with a variable density. Taking into account the influence of
DEV on the universe expansion we find the value of $\alpha$ which could remove
the HT problem. In order to maintain the almost constant DEV/DM energy density
ratio during the time interval at $z<1100$, we suggest an existence of a wide
mass DM particle distribution.
