  Among many models which can describe the bouncing cosmology, A matter bounce
scenario that is deformed by a running vacuum model of dark energy (RVM-DE) has
been interested. In this research, I show that a class of RVM-CDM (cold dark
matter) model can also describe a cyclical cosmology in which the universe
undergoes cycles of expansion to the contraction phase and vice versa. To this
end, following our previous work, I consider one of the most successful class
of RVM-CDM model in bouncing cosmology, $\rho_x=n_0+n_2 H^2 +n_4 H^4$, in which
the power spectral index gets a red tilt and the running of the spectral index
may give a negative value by choosing the appropriate value of parameters
($n_0,~n_2,~n_4$), which is consistent with the cosmological observations. It
is worthwhile to mention that most matter bounce models do not produce this
negative value. However, the main purpose of this article is to investigate the
RVM-CDM model in the turnaround phase. Far from the bounce in a phantom
expanding universe, the turnaround conditions are investigated before the
occurrence of a sudden big rip. By analyzing the Hubble parameter, equation of
state parameter, and deceleration parameter around the turnaround, we show that
a successful turnaround may occur after an expansion in an \textbf{interacting}
case of RVM-CDM by choosing the appropriate value of parameters. A minimum
value for the interaction parameter is obtained and also finds any relation
between other model parameters. Finally, the effect of each parameter on a
turnaround is studied, and we see that the transition time from accelerating to
decelerating expansion can occur earlier for larger values of interaction
parameters. Also, in several graphs, the effect of the second term in DE
density, including $H^2$, is studied, and we see that by increasing its
coefficient, $n_2$, the transition point leads to lower values.
