The source 4U 1812-12 is a persistent, weakly variable low-mass X-ray binary containing a neutron star. The source was observed by NICER between 2019 and 2021 and, more recently, by NuSTAR in 2025. During the NICER and NuSTAR observations, the source was detected in a hard spectral state with a bolometric luminosity of ∼1.90×1036 ergs s−1. Its 3−70
Nearby in the stack
keV NuSTAR spectrum is characterized by a soft thermal emission from the disc, a hard Comptonized emission from the corona, and its reflection from the accretion disc. The NuSTAR energy spectrum exhibits the clear presence of disc reflection features, fitted using a self-consistent relativistic reflection model relxill. Our reflection modeling indicates a moderately ionized accretion disc (log
ξ∼2.72
) extending close to the neutron star surface (
Rin≲1.72RISCO
), and viewed through a small inclination angle (
i∼25
degrees). Assuming that the magnetic field (
B
) truncates the disc, we found
B≲2.54×108
G, comparable to the typical values observed for NS LMXBs. The
1.0−9.5
keV NICER spectra are also characterized by a soft thermal component and a dominant hard Comptonized component. During NICER observations, the disc temperature exhibits a small variation within
∼0.69−0.84
keV. In contrast, the power law photon index,
Γ
, exhibits a large variation of
∼0.8−1.5
, implying a substantial change in the Comptonized emission. Moreover, NICER timing analysis reveals broadband aperiodic variability with significant QPO-like features at