  Recently, repeating fast radio bursts (FRBs) with a period of $P_{\rm
FRB}=16.35\pm0.18$ days from FRB 180916.J0158+65 had been reported. It still
remains controversial how to give rise to such a periodicity of this FRB. In
this Letter, based on an assumption of a young pulsar surrounding by a debris
disk, we attempt to diagnose whether the Lense-Thirring precession of the disk
on the emitter can produce the observed periodicity. Our calculations indicate
that the Lense-Thirring effect of a tilted disk can result in a precession
period of 16 days for a mass inflow rate of $0.5-1.5\times10^{18}~\rm
g\,s^{-1}$, a spin period of 1-20 ms of the pulsar, and an extremely low
viscous parameter $\alpha=10^{-8}$ in the disk. The disk mass and the magnetic
field of the pulsar are also constrained to be $\sim10^{-3}~\rm M_{\odot}$ and
$< 2.5\times 10^{13}~\rm G$. In our model, a new born pulsar with normal
magnetic field and millisecond period would successively experience accretion
phase, propeller phase, and is visible as a strong radio source in the current
stage. The rotational energy of such a young NS can provide the observed radio
bursting luminosity for $400$ years.
