  Recent observational and numerical studies show a variety of thermal
structures in the solar chromosphere. Given that the thermal interplay across
the transition region is a key to coronal heating, it is worth investigating
how different thermal structures of the chromosphere yield different coronal
properties. In this work, by MHD simulations of Alfv\'{e}n-wave heating of
coronal loops, we study how the coronal properties are affected by the
chromospheric temperature. To this end, instead of solving the radiative
transfer equation, we employ a simple radiative loss function so that the
chromospheric temperature is easily tuned. When the chromosphere is hotter,
because the chromosphere extends to a larger height, the coronal part of the
magnetic loop becomes shorter, which enhances the conductive cooling. A larger
loop length is therefore required to maintain the high-temperature corona
against the thermal conduction. From our numerical simulations we derive a
condition for the coronal formation with respect to the half loop length
$l_{\rm loop}$ in a simple form: $l_{\rm loop} > a T_{\rm min} + l_{\rm th}$,
where $T_{\rm min}$ is the minimum temperature in the atmosphere and parameters
$a$ and $l_{\rm th}$ have negative dependencies on the coronal field strength.
Our conclusion is that the chromospheric temperature has a non-negligible
impact on coronal heating for loops with small length and weak coronal field.
In particular, the enhanced chromospheric heating could prevent the formation
of the corona.
