  It is accepted in modern cosmology that the scalar field responsible for the
inflationary stage of the early Universe is completely transformed into matter.
It is assumed that the accelerated expansion is currently driven by dark energy
(DE), which is likely determined by Einstein's cosmological constant. We
consider a cosmological model where DE can have two components, one of which is
Einstein's constant ($\Lambda$) and the other, smaller variable component DEV
($\Lambda_V$), is associated with the remnant of the scalar field that caused
inflation after the main part of the scalar field has turned into matter. It is
assumed that such a transformation continues at the present time and is
accompanied by the reverse process of the DM transformation into a scalar
field. The interconnection between DM and DEV, which leads to a linear
relationship between the energy densities of these components after
recombination $\rho_{DM}=\alpha\;\rho_{DEV}$, is considered. Variants with a
dependence of the coefficient $\alpha(z)$ on the redshift are also considered.
One of the problems that have arisen in modern cosmology, called Hubble Tension
(HT), is the discrepancy between the present values of the Hubble constant
measured from observations at small redshifts $z\lesssim1$ and the values found
from fluctuations of the cosmic microwave background at large redshifts
$z\approx1100$. In the considered model, this discrepancy can be explained by
the deviation of the real cosmological model from the conventional cold dark
matter (CDM) model of the Universe by action of the additional DE component at
the stages after recombination. Within this extended model, we consider various
$\alpha(z)$ functions that can eliminate the HT. To maintain the ratio of DEV
and DM energy densities close to constant over the interval $0\le z\le1100$, we
assume the existence of a wide spectrum of DM particle masses.
