  We present a thorough study of the Changing-Look Active Galactic Nucleus
(CL-AGN) Mrk 1018, utilizing an extensive dataset spanning optical, UV, and
X-ray spectro-photometric data from 2005 to 2019. We analysed X-ray spectra and
broad-band photometry, and performed optical-to-X-ray spectral energy
distribution (SED) fitting to comprehend the observed changing-look behaviour.
We found that over the 14 years in analysis, significant changes in X-ray
spectra occurred, as the hardness ratio increases by a factor of ~2. We
validated also the broad-band dimming, with optical, UV, and X-ray luminosities
decreasing by factors of >7, >24 and ~9, respectively. These dims are
attributed to the declining UV emission. We described the X-ray spectra with a
two-Comptonization model, revealing a consistent hot comptonizing medium but a
cooling warm component. This cooling, linked to the weakening of the magnetic
fields in the accretion disk, explains the UV dimming. We propose that the
weakening is caused by the formation of a jet, in turn originated from the
change of state of the inner accretion flow. Our optical-to-X-ray SED fitting
supports this conclusion, as the normalised accretion rate is super-critical
($\mu=$0.06>0.02) in the bright state and sub-critical ($\mu=$0.01<0.02) in the
faint state. Instabilities arising at the interface of the state-transition are
able to reduce the viscous timescale to the observed ~10 years of Mrk 1018
variability. We explored a possible triggering mechanism for this state
transition, involving gaseous clouds pushed onto the AGN sub-pc regions by a
recent merging event or by cold chaotic accretion. This scenario, if validated
by future simulations, could enhance our understanding of CL-AGN and raises
questions about an accretion rate of ~0.02, coupled with minor disturbances in
the accretion disk, being the primary factor in the changing-look phenomenon.
