The young pulsars mostly locate in the supernova remnants, which can be classified as the rotation-powered pulsars, magnetars and central compact objects, and these three types of young pulsars share the different distributions of the spin periods and magnetic field strengths. The remnant magnetars share the average spin period larger than the rotation-powered remnant pulsars by nearly one order of magnitude, while their average magnetic field strength is higher than that of the rotation-powered remnant pulsars by about two orders of magnitude. Meanwhile, the central compact objects share the average magnetic field strength lower than the rotation-powered remnant pulsars by about two orders of magnitude. The different physical properties of these three types of young pulsars may originate from their different predecessors, or their different supernova processes, and may also originate from their different evolutional processes after the neutron stars were born. Furthermore, the rotation-powered remnant pulsars exhibit the faster average spin period, the higher average magnetic field strength, and the shorter average characteristic age than the young rotation-powered non-remnant pulsars. This implies that when the new born neutron star undergos the evolution process with the timescale of $\tau\sim10^5-10^6$ yr, its spin velocity will decrease by about a half, and its magnetic field strength will also decrease by about a half simultaneously.