  We present the results of photometric and spectroscopic monitoring campaigns
of the changing look AGN NGC~2617 carried out from 2016 until 2022 and covering
the wavelength range from the X-ray to the near-IR. The facilities included the
telescopes of the SAI MSU, MASTER Global Robotic Net, the 2.3-m WIRO telescope,
Swift, and others. We found significant variability at all wavelengths and,
specifically, in the intensities and profiles of the broad Balmer lines. We
measured time delays of ~ 6 days (~ 8 days) in the responses of the H-beta
(H-alpha) line to continuum variations. We found the X-ray variations to
correlate well with the UV and optical (with a small time delay of a few days
for longer wavelengths). The K-band lagged the B band by 14 +- 4 days during
the last 3 seasons, which is significantly shorter than the delays reported
previously by the 2016 and 2017--2019 campaigns. Near-IR variability arises
from two different emission regions: the outer part of the accretion disc and a
more distant dust component. The HK-band variability is governed primarily by
dust. The Balmer decrement of the broad-line components is inversely correlated
with the UV flux. The change of the object's type, from Sy1 to Sy1.8, was
recorded over a period of ~ 8 years. We interpret these changes as a
combination of two factors: changes in the accretion rate and dust recovery
along the line of sight.
