  We present ALMA observations of the [CII] 158 $\mu$m fine structure line and
dust continuum emission from two quasars, SDSS J104433.04-012502.2 and SDSS
J012958.51-003539.7, at z=5.78. The ALMA observations at 0.2'' resolution map
the dust and gas on kpc scales. The spatially resolved emission shows a similar
trend of decreasing [CII]-FIR ratios with increasing FIR surface brightnesses
as was found in the infrared luminous galaxies with intense star formation. We
confirm the velocity gradients of [CII] emission found previously in SDSS
J0129-0035. No clear evidence of order motion is detected in SDSS J1044-0125.
The velocity maps and PV-diagrams also suggest turbulent gas clumps in both
objects. We tentatively detect a [CII] peak offset 4.9 kpc to the East of SDSS
J1044-0125. This may be associated with an infalling companion, or node of gas
outflow. All these results suggest significant dynamical evolution of the ISM
in the nuclear region of these young quasar-starburst systems. We fit the
velocity map of the [CII] emission from SDSS J0129-0035 with a rotating disk
model. The result suggests a face-on system with an inclination angle of 16 +/-
20 degree and constrains the lower limit of the host galaxy dynamical mass to
be 2.6x10^10 Msun within the [CII] emitting region. It is likely that SDSS
J0129-0035, as well as other young quasars with super massive black hole masses
on order of 10^7 to 10^8 Msun, falls close to the black hole and host galaxy
mass relation defined by local galaxies.
