We present extensive, well-sampled optical and ultraviolet photometry and optical spectra of the Type Ia supernova (SN Ia) 2017hpa. The light curves indicate that SN 2017hpa is a normal SN Ia with an absolute peak magnitude of $M_{rm max}^{B} approx$ -19.12$pm$0.11 mag and a post-peak decline rate mb = 1.02$pm$0.07 mag. According to the quasibolometric light curve, we derive a peak luminosity of 1.25$times$10$^{43}$ erg s$^{-1}$ and a $^{56}$Ni mass of 0.63$pm$0.02 $M_{odot}$. The spectral evolution of SN 2017hpa is similar to that of normal SNe Ia, while it exhibits unusually rapid velocity evolution resembling that of SN 1991bg-like SNe Ia or the high-velocity subclass of SNe Ia, with a post-peak velocity gradient of $sim$ 130$pm$7 km s$^{-1}$ d$^{-1}$. Moreover, its early spectra ($t < -7.9$ d) show prominent CII~$lambda$6580 absorption feature, which disappeared in near-maximum-light spectra but reemerged at phases from $t sim +8.7$ d to $t sim +11.7$ d after maximum light. This implies that some unburned carbon may mix deep into the inner layer, and is supported by the low CII~$lambda$6580 to SiII~$lambda$6355 velocity ratio ($sim 0.81$) observed in SN 2017hpa. The OI~$lambda$7774 line shows a velocity distribution like that of carbon. The prominent carbon feature, low velocity seen in carbon and oxygen, and large velocity gradient make SN 2017hpa stand out from other normal SNe Ia, and are more consistent with predictions from a violent merger of two white dwarfs. Detailed modelling is still needed to reveal the nature of SN 2017hpa.
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