  G213.0$-$0.6 is a faint extended source situated in the anti-center region of
the Galactic plane. It has been classified as a shell-type supernova remnant
(SNR) based on its shell-like morphology, steep radio continuum spectrum, and
high ratio of [S II]/H$\alpha$. With new optical emission line data of
H$\alpha$, [S II], and [N II] recently observed by the Large Sky Area
Multi-Object Fiber Spectroscopic Telescope, the ratios of [S II]/H$\alpha$ and
[N II]/H$\alpha$ are re-assessed. The lower values than those previously
reported put G213.0$-$0.6 around the borderline of SNR-HII region
classification. We decompose the steep-spectrum synchrotron and the
flat-spectrum thermal free-free emission in the area of G213.0$-$0.6 with
multi-frequency radio continuum data. G213.0$-$0.6 is found to show a flat
spectrum, in conflict with the properties of a shell-type SNR. Such a result is
further confirmed by TT-plots made between the 863-MHz, 1.4-GHz, and 4.8-GHz
data. Combining the evidence extracted in both optical and radio continuum, we
argue that G213.0$-$0.6 is possibly not an SNR, but an HII region instead. The
$V_{LSR}$ pertaining to the H$\alpha$ filaments places G213.0$-$0.6
approximately 1.9 kpc away in the Perseus Arm.
