  We use X-ray and infrared observations to study the properties of three
classes of young stars in the Carina Nebula: intermediate-mass (2--5~M$_\odot$)
pre-main sequence stars (IMPS; i.e. intermediate-mass T Tauri stars), late-B
and A stars on the zero-age main sequence (AB), and lower-mass T Tauri stars
(TTS). We divide our sources among these three sub-classifications and further
identify disk-bearing young stellar objects versus diskless sources with no
detectable infrared (IR) excess emission using IR (1--8 $\mu$m) spectral energy
distribution modeling. We then perform X-ray spectral fitting to determine the
hydrogen absorbing column density ($N_{\rm H}$), absorption-corrected X-ray
luminosity ($L_{\rm X}$), and coronal plasma temperature ($kT$) for each
source. We find that the X-ray spectra of both IMPS and TTS are characterized
by similar $kT$ and $N_{\rm H}$, and on average $L_{\rm X}$/$L_{\rm bol}
\sim4\times10^{-4}$. IMPS are systematically more luminous in X-rays (by
$\sim$0.3 dex) than all other sub-classifications, with median $L_{\rm X} =
2.5\times10^{31}$ erg s$^{-1}$, while AB stars of similar masses have X-ray
emission consistent with TTS companions. These lines of evidence converge on a
magneto-coronal flaring source for IMPS X-ray emission, a scaled-up version of
the TTS emission mechanism. IMPS therefore provide powerful probes of
isochronal ages for the first $\sim$10 Myr in the evolution of a massive
stellar population, because their intrinsic, coronal X-ray emission decays
rapidly after they commence evolving along radiative tracks. We suggest that
the most luminous (in both X-rays and IR) IMPS could be used to place empirical
constraints on the location of the intermediate-mass stellar birth line.
