  We made use high-cadence observations from the $Insight$-HXMT and $NICER$ to
scrutinize the spectral and timing evolution during the 2018 outburst of the
black hole X-ray binary (BHXRB) MAXI J1820+070. It's hardness-intensity diagram
(HID) displays a ''q''-like track including all the spectral states, along a
unique loop in the hard state. The tracks observed in the HID is anticipated in
the evolution of the components responsible for Compton and reflection
emission. This is substantiated by the relationship between the X-ray
luminosity $L_\mathrm{X}$ and photon index $\Gamma$, as well as the
relationship between X-ray luminosity $L_\mathrm{X}$ and the ratio of Compton
to disk luminosities $L_\mathrm{C}/L_\mathrm{D}$. Both of these relationships
exhibit a pattern reminiscent of HID. During the hard state, the hardness (also
$\Gamma$) is determined by either reflection component ($R_{f}>1$ ) or Compton
component ($R_{f}<1$) depending on the value reflection fraction $R_{f}$. So
the distinctive evolution of $R_{f}$ leads to the unique loop in the HID (also
in the $L_\mathrm{X}$--$\Gamma$ plane) of hard state. Additionally, we found a
negative correlation between frequency of the type-C quasi-periodic oscillation
(QPO) ($\nu_{\mathrm{C,QPO}}$) and the optical depth of the Compton emission
($\tau$), and a positive correlation between $\nu_{\mathrm{C,QPO}}$ and
$\Gamma$. These correlations strongly suggest a coupling between the QPO
properties and the underlying process responsible for Comptonization.
